DRS USER MANUAL Doc. No. 3M6-MAN-HAR-33110-0016
Contents
1. wem ES s 4 3 5 TH resulttbl 4 3 6 drift resulttbl T3 5 COE ar bp Soo ds 44 Databases RE RS 4 4 1 Calibration Database 4 4 2 Reduction Performance list 4 4 3 Intrument Configuration DataPool 4 4 4 Intrument Performance Database 5 Off line DRS Description 91 Overview ke vo o es Det RECIPE SERIES AS o RR Rd og 3M6 MAN HAR 33110 0016 Issue 1 0 5 2 1 off visu 20 5 2 20 5 2 2 off visu 51 Display SID spectrum 29 5 2 3 Off visu cer Display Br DDr 30 5 24 off 1 5 _ 30 5 2 5 off visu Display RV per Orders 30 5 2 6 off newccf Re process CCF 31 6 Use of the Data Archiving Unit 33 vi 3M6 MAN HAR 33110 0016 Issue 1 0 Chapter 1 Introduction 1 1 Scope HARPS is a spectrograph dedicated to the search for extra solar planets by means of the technique of precise radial velocity measurement HARPS is developed by a consortium headed by the Geneva Observatory It is installed at the Coud room of the 3 6 m ESO telescope at La Silla with an optical fiber link to the Cassegrain focus The present document describes the Dat2. For thorium spectrum an extension wave is also produced by the DRS It is a e2ds format image where the matrix stores the wavelength value of each pixel instead of the flux of the spectrum 4 2 7 Extracted one dimensional spectra 614 The extracted one dimensional spectra S1D is a real vector written on disk in FITS format with the _51 suffix added to the generic name This vector contains the rebinned and merged spectral orders in relative flux corrected from the instrumental respond and stretched to the barycentric referential The wavelength step is 0 01 Angstrom 4 2 8 Cross correlation function ccf The cross correlation function is stored with the suffix cc template name with template name the file name of the corresponding template also called coorelation mask used to compute it The matrix is made of Norder CCF spectrum corresponding to the CCF computed for each order The following extra descriptor HIERARCH ESO DRS related to CCF are included CCF MASK template filename CCF MAXCPP max count pixel in the continuum of the CCF e CCF FWHM FWHM of CCF km s gaussian fit CCF RV Baryc Rad vel km s gaussian fit CCF LINES nbr of lines used by the template CCF CONTRAST Contrast of CCF gaussian fit BERV Barycentric Earth Radial Velocity correction BJD Barycentric Julian Day BERVMX Maximum BERV along the year DRIFT REF FILE Th Drift ref file used string DRIFT VR Th RV Drift m s float 3M6
3. Read the last localisation in the Calibration Data Base Horn optimum extraction of orders box window is used to smooth the tungsten flux along the orders to determine a pseudo blaze response Divide the extracted tungsten spectrum by this blaze response to obtain the flat field spectrum Computation of the SNR at the blaze center and the dispersion of the flat field The Blaze for each orders is stored in a FITS file with the suffix blaze The Flat for each orders is stored in a FITS file with the suffix 1at Parameters of 3 orders are appended in the file cal FF result tbl If passed Quality control update the Calibration Data Base 12 3M6 MAN HAR 33110 0016 Issue 1 0 Outputs Ascii cal FF result tbl Fits files generic name blaze A fits and generic name blaze B fits Fits files generic name flat A fits and generic name flat B fits Quality control check staturation level stop DRS if saturated check FF parameters rms 0 033 e S N 100 CalibDB is not updated if failed 3 20 5 cal TH Thorium Calibration Inputs Raw fits frame obtained with the HARPS ech cal thoAB template Description Retrieve from calibDB previous last full calibration sets Correction of the bad columns of the CCDs average of adjacent columns Correction of the BIAS as described previously Fit on raw frame a small set of thorium lines and save parameters in a tbl file with suffix spot_thAB Read th
4. err posx 161 fwhm 161 err fwhm 161 posx 114 err posx 114 fwhm 114 err fwhm 114 posx 89 err posx 89 fwhm 89 err fwhm 89 name of the night directory name of the corresponding raw frame CCD read out mode dark exposure time s mean dark level e hour number of cosmic events event cm2 mn 4 3 3 cal loc ONE result tbl name of the night directory name of the corresponding raw frame fiber name A or B location of the center of the order 161 pixel error on order location pixel width of the center of the order 161 pixel error on the width of the center of the order 161 pixel same than above for order 114 same than above for order 114 same than above for order 114 same than above for order 114 same than above for order 89 same than above for order 89 same than above for order 89 same than above for order 89 3M6 MAN HAR 33110 0016 Issue 1 0 25 4 3 4 cal FF result tbl column description night name file name nbfi les fi ber FFrms 161 S N 161 FFrms 114 S N 114 FFrms 89 S N 89 name of the night directory name of the corresponding raw frame number of frame coadded fiber name A or B rms on the flat field at center of order 116 S N ratio per extracted pixel at center of order 161 same than above for order 114 same than above for order 114 same than above for order 89 same than above for order 89 4 3 5 cal TH result tbl column description night name file name
5. fi ber fiber A or B mask Name of the ccf template maxccp Maximum of count per pixel in the CCF 3M6 MAN HAR 33110 0016 Issue 1 0 24 lines Number of spectral lines used in the CCF contrast Contrast of the CCF 96 RV RV km s corrected from BERV FWHM FWHM of the CCF km s 4 4 Databases Several Databases are accessed by the DRS The DRS uses Calibrations Databases to store and to retrieve calibrations Its needs a Reduction Performance List for the quality control The DRS main engine uses the Instrument Confi guration Data Pool as input reference to carry on the reduction 4 4 1 Calibration Database The Calibration Databases includes all relevant calibrations which have passed properly the quality control tests It contains BIAS frames DARK frames localization images flat fields and thorium calibrated spectra A master calib tbl file keeps track of all the calibration frames All calibration frames needed and accessed by the DRS during the reduction process are automatically copied on the directory where all data product of the DRS are stored This allow the observer to have a self consistent set of data products if he wants to reprocess his observations Calibration Database stores a full calibration set made of e order localisation A and B e flat field and blaze spectrum A and B e wavelenth solution A and B e reference thorium spectrum B 4 4 2 Reduction Performance list The reduction performance
6. MAN HAR 33110 0016 Issue 1 0 23 DRIFT NBCOS Th Drift Nbr cosmic detected integer DRIFT RFLUX Th Drift Flux ratio float DRIFT NBORDKILL Th Drift Nb orders killed integer DRIFT NOISE Th Drift photon noise m s float 4 3 Summary tables The DRS produces a set of summary table for performance tracking of calibration exposure The tables have ASCII format with a TAB for separator BIAS result tbl for BIAS cal DARK result tbl for DARK cal loc ONE result tbl for the order localization FF result tbl for Flat Field TH result tbl for thorium calibration drift result tbl for instrumental drift CCF result tbl for CCF 4 3 1 cal BIAS result tbl column description night name name of the night directory file name name of the corresponding raw frame ccd mode CCD read out mode mean biasl mean bias in zone 1 prescan Linda ADU rms biasl rms bias in zone 1 prescan Linda ADU mean bias2 mean bias in zone 2 overscan Linda ADU rms bias2 rms bias in zone 2 overscan Linda ADU mean bias3 mean bias in zone 3 prescan Jasmin ADU rms bias3 rms bias in zone 3 prescan Jasmin ADU mean bias4 mean bias in zone 4 overscan Jasmin ADU rms bias rms bias in zone 4 overscan Jasmin ADU 24 3M6 MAN HAR 33110 0016 Issue 1 0 4 3 2 cal DARK result tbl column description night name file name ccd mode dark time mean dark cosmic column description night name file name fi ber posx 161
7. click on the Go button to start the backup Files are then copied in the wharch workstation under the BACKUP directory 4 De select the backup button and check that the Size is less than 4400 MB 5 Put a writable DVD in the burner 6 Select the Prepare DVD and Write DVD button 7 Click the button to start archiving If the total data size is too big for one DVD more than 4 4 GBytes the raw files will be automatically compressed by about 50 approximately 170 gzipped FITS files fit on one DVD If the volume is still too large the user has to split the night in two e g lt night gt a and lt night gt _b directories To archive both directories the complete name of the directory has to be put in the Night field Both directories have to be archived separately The Compute size button computes the total size of the data saved in the BACKUP under the lt night gt directory 33 34 3M6 MAN HAR 33110 0016 Issue 1 0 APPENDIX Fiber A Fiber B Grating Central order order order 0 0 161 1 1 160 2 2 159 44 44 117 45 GAP 116 GAP 115 46 45 114 47 46 113 70 69 90 71 70 89 wavelength 3802 3826 3850 A 5232 5277 5318 5370 5417 6801 A 6877 Table 6 1 Order identified and extracted by DRS
8. of the bad columns of the CCDs average of adjacent columns Measurement of the mean level and the dispersion of the 4 overscan areas Measurement of the mean level and the dispersion of the 4 CCD ports Print and Display of the results Store results on the cal BIAS result tbl Outputs Ascii file cal BIAS result tbl 10 3M6 MAN HAR 33110 0016 Issue 1 0 Quality control Quality control with warning message when bias level 500 ADU or bias noise 10 e 3 2 2 cal DARK CCD Dark Inputs Raw fits frame obtained with the HARPS ech cal dark template Description Read keywords related to the CCDs parameters readout mode readout noise gain Correction of the bad columns of the CCDs average of adjacent columns Mean level and dispersion of the Bias on the 4 overscan areas Mean level and dispersion of the 4 CCD ports with sigma clipping of the cosmic hits Calculation of the mean dark level e hour Calculation of the number of cosmic events event cm2 mn Store result on the file ca1 DARK result tbl Outputs Ascii cal DARK result tbl Quality control Error message if the exposure time is shorter than 5 minutes DRS stoppped Warning if dark level gt 10 e hour or cosmic events gt 10 event cm2 mn 3 2 3 cal loc ONE Geometry of orders of One fiber Inputs Two raw fits frames obtained from a sequence of two successive Tungsten exposures with the HARPS ech cal tun te
9. 3 to 4 pixels The position x of the center of each orders for each rows y is stored in a FITS file with the suffix loco The FWHM of each orders for each rows y is stored in a FITS file with the suffix fwhm order Parameters of 3 orders are appended in the file 1 1oc ONE result tbl Quality control on the number of orders identified dispersion of the center and FWHM If passed the Quality control updates the Calibration Data Base Outputs Ascii cal 1oc ONE result tb l Fits files generic name 1 A fits and generic name loco B fits Fits files generic name whm order A fits and generic name fwhm order B fits Quality control Error if flux level on the central row 65000 ADU Flux 15000 ADU DRS stops Quality control on the number of orders 72 71 dispersion of the fit both on center and FWHM values of order profiles 0 1 pix If Quality control fails calibDB is not updated 3 20 4 cal FF Flat field measurement Inputs Several raw fits frames obtained from a sequence of Tungsten exposures on the two fibers with the HARPS ech cal tunAB template or HARPS ech tunUSER at least 5 frames in order to reach the photon noise level above the flat field noise Description Retrieve from calibDB previous last full calibration sets Sum of the raw frame delivered Correction of the bad columns of the CCDs average of adjacent columns Correction of the BIAS as described previously
10. Planeta Searc EUROPEAN SOUTHERN OBSERVATORY OBSERVATOIRE DE GEN VE OBSERVATOIRE DE HAUTE PROVENCE p UNIVERSITAT BERN SERVICE D A RONOMIE OBSERVATOIRE DE GENEVE 51 CH DES MAILLETTES CH 1290 SAUVERNY SWITZERLAND PHONE 41 0 22 755 26 11 Fax 41 0 22 755 39 83 HARPS DRS USER MANUAL Doc No 3M6 MAN HAR 33110 0016 Issue 1 0 30 september 2003 Prepared F Bouchy D Queloz 30 09 2003 7 Signature Approved D M gevand 42 ee ewe Gea eee eS Date Signature Released Mayor Date Signature 3M6 MAN HAR 33110 0016 Issue 1 0 Change Record Section Page affected Reason Remarks Ho famo ii 3M6 MAN HAR 33110 0016 Issue 1 0 Contents 1 Introduction 1 L SCOPES che Od a a ee He LR SCR o Rome UN 1 1 2 s Applicable Documents i es 22 22 44 pod egg goal bu AI Re 1 1 3 Abbreviations and Acronyms 2 2 DRS Hardware and Software Environment 3 21 Overview uos eov Sor doe ar OES alae Oe beet 3 2 2 Architecture of the data on WHADRS 3 2 3 Execution of the On line DRS 3 2 4 Execution of the Off line DRS 6 2 9 Programming language moe EP qe AR RECS SSH EERE ges pes 6 2 6 Architecture of the DRS 7 2 7 Architecture of the DRS Modules 7 3 On line D
11. RS Description 9 Al OVERVIEW ou y Y OY A MEN Y Ee dk ck Pk cede P MAS 9 22 RECIPES 2 2 24 was VES PEASE ee EE 9 32 cal BIAS CCD BIAS vos a y vex SO OY ORE RE Y oe x 9 322 seal DARK CCD D tk ii XXE XD EUR NDA 10 3 2 3 cal loc ONE Geometry of orders of One 10 3 24 FF Flat field measurement 11 3 2 5 cal TH Thorium Calibration 12 3 2 6 cal I2 I spectrum measurement 13 3 2 7 obj_TH Accurate RV measurement i 42 32 2224282224 32 8272854 13 iii iv 3M6 MAN HAR 33110 0016 Issue 1 0 3 2 8 obj ONE Spectroscopy using One fiber 3 2 9 obj TWO Spectroscopy using Two fibers 4 DRS Data Product Description 4 1 4 22 421 22 4 gt 4 2 2 Localization frames loco _fwhm order_ 4 023 Flat field frames flat 424 Blaze frames blaze 4 2 5 Wavelength frames wave 4 2 6 Extracted two dimensional spectra e2ds 4 27 Extracted one dimensional spectra_sld_ 4 2 8 Cross correlation function_ccf_ 4 3 Summary tables 4 32 2 4 SS VARESE TENS 4 3 1 cal BIAS result tbl 4 3 2 cal DARK resulttbl 4 3 3 cal loc ONE resulttbl ASA Cal FE
12. SSS fits raw frame Tables in ASCII format are also produced by the DRS See in Table TBC for a list and a description of the content of tables The relevant log books of the DRS is named DRS whadrs YYYY MM DD 4 0 Data formats 4 2 1 Raw frames The raw frame corresponds to a 4296 x 4096 integer 35 242 560 bytes matrix written on disk in FITS format see Fig 4 1 This images includes a 4096x4096 sensitive zone plus 4 over and prescan zone of 50 pixels each The following generic descriptors are used by the DRS DATE OBS Date and Time of beginning of observation string RA RA of the target float DEC DEC of the target float 17 18 3M6 MAN HAR 33110 0016 Issue 1 0 The DRS needs as well the following HIERARCH ESO descriptors DET READ SPEED CCD Readout mode speed port and gain string DET OUT2 RON Readout noise e of Linda Blue float DET OUT2 CONAD Conversion from ADUs to electrons of Linda Blue float DET OUT4 RON Readout noise e of Jasmin Red float DET OUT4 CONAD Conversion from ADUs to electrons of Jasmin Red float DET WIN1 DIT1 Actual sub integration time s float DET WIN1 DKTM Dark current time s float DET DPR CATG Observation category string DET DPR TYPE Exposure type string INS DET1 TMMEAN Normalised mean exposure time float INS DET1 CMMEAN Average count PM on fiber A float INS DET2 CMMEAN Average count PM on fiber B float OBS TARG NAME T
13. a Reduction Software DRS as well as its current architecture and configuration The reader is supposed to be familiar with all the applicable documents listed below Chapter 2 describes the Hardware and Software environment of the DRS Chapter 5 describes programs modules and functions of the DRS Chapter 4 describes the data used and produced by the DRS 1 2 Applicable Documents The following documents of the exact issue shown form a part of this document to the extent speci fied herein 1 2 3M6 SPE HAR 33100 0002 2 0 31 05 2002 HARPS Tech Requirements Spec 3M6 PLA HAR 33100 0005 1 4 11 06 2001 HARPS Oper Calib and Maint Plan 3M6 TRE HAR 33110 0005 1 1 10 07 2001 HARPS DFS Design Description 4 3M6 TRE HAR 33110 0006 1 0 09 06 2001 HARPS DRS Design Description 5 3M6 TRE HAR 33110 0019 1 0 12 12 2002 HARPS DRS Test and Progress Report 6 3M6 TRE HAR 33110 0008 1 31 22 01 2002 Templates Reference Guide 3 1 3 2D AFPO CCD CCF CDB DAU DFS DRS E2DS ESO GUI ICDP LED LSO MS OG OS QC QE RMS RON RV RVPO SID SNR SW TBD TBC VLT Abbreviations and Acronyms Two Dimension Average Flux per order Charge Coupled Device Cross Correlation Function Calibration Database Data Archiving Unit Data Flow System Data Reduction Software Extracted 2 Dimension Spectra European Southern Observatory Graphical User Interface Instrument Configuration Data Pool Light Emitting Diode ESO Chi
14. arget name string TEL TARG EQUINOX Equinox float TEL TARG PMA Proper motion alpha arcsec year float TEL TARG PMD Proper motion delta arcsec year float TEL TARG RADVEL Radial velocity of target km s float TEL AMBI FWHM START seeing at start float TEL AMBI FWHM END seeing at end float TEL AIRM START air mass at start float TEL AIRM END air mass at end float TPL NEXP TPL Number of exposures integer TPL EXPNO TPL Exposure number within template integer TPL NAME TPL NAME string 3M6 MAN HAR 33110 0016 Issue 1 0 19 x 4296 y 4096 SS x 4296 y 1 x 4296 columns JASMIN CCD LINDA CCD x 1 y 4096 4096 raws x 1 y 1 Figure 4 1 Raw frame format The raw image is oriented in order to correspond to the CCD orienta tion in focal plane when looking at the detector from the spectrograph 4 2 2 Localization frames loco and fwhm order _ Centers and FWHM of orders are stored in two 4096 x Norder real matrix written on disk in FITS format with the suffix 1 and fwhm order added to the generic name Each lines corresponds to an order and each column to a line of the CCD raw frame The localization frame loco contains the position of the center positions of orders The localization frame whm order contains the FWHM of orders Pay attention to the orientation of the raw frame by comparison with the E2DS format described below The FITS descriptor includes all descript
15. at field sequence l 1 1 FF Wavelength calibration li b spectrum measurement Science Observations Accurate RV measurement acq_thosin Spectroscopy Io acq I2cell Spectroscopy for object only acq_objA Spectroscopy object and sky objAB Table 2 1 List of on line data reduction programs night directory name Y Y Y Y MM DD raw frame name s HARPS Y Y Y Y MM DDTHH MM SS SSS fits for some recipes a list of raw frame names is needed For example the command cal loc ONE py 2002 02 11 HARPS 2002 02 11T20 13 45 768 fits reduces the raw frame HARPS 2002 02 11T20 13 45 768 fits with the reduction program cal loc ONE The raw frame is read in the directory data raw 2002 02 11 and all DRS products are stored in the directory data reduced 2002 02 11 The logs of the DRS are stored in the file data msg DRS whadrs 2002 02 11 The list of the raw frames obtained on a night is stored in the data msg 2002 02 11 r The reduction programs are executable files actually python scripts that contain all relevant infor mation to carry out the reduction No other parameters nor options are needed for the reduction Parameters specific to the exposure are in the FITS descriptors of the raw frame The Trigger runs automatically the appropriate reduction program of each frame or set of frames as soon as the exposure is archived and available on the DRS machine The reduction
16. e last localisation and flat field in the Calibration Data Base Horn optimum extraction of orders Flat field correction Compute the RV drift from the last Th Calibration in the Calibration Data Base Identify lines using calibration provided by calibDB if calibration is not available first wavelength calibration procedure must be used Fit each thorium emission line Adjust a polynomial solution for each order with a sigma clipping scheme Compute the Littrow first and second order deviation and computes the granulation of the global solution Save E2DS Thorium spectrum in FITS file with the suffix e2ds with all descriptors Save an image of the wavelength solution wavelength of each orders for each pixels in FITS file with the suffix wave Parameters of the Thorium wavelength calibration are appended in the file cal TH result tbl Listing of all Thorium lines detected are stored in a tbl file with suffix th 1ines If passed Quality control update the Calibration Data Base Outputs Ascii cal TH result tb l Ascii file generic name spot thAB tbl Ascii file generic name th lines A tbl Ascii file generic name th lines B tbl Fits files generic name e2ds A fits and generic name e2ds B fits Fits files generic name wave A fits and generic name wave B fits Quality control 3M6 MAN HAR 33110 0016 Issue 1 0 13 Check if Littrow solution has rms granulation less 50m s
17. ed spectrum SID and save it with the suffix s1d Compute the Barycentric Earth Radial Velocity Compute the cross correlation function with a template mask driven by the spectral type and save the average CCF in the fits file generic name ccf mask A fits the RV for each orders in the table generic name cc mask A tb1 and the summary of results on the table CCF_result tbl Outputs Ascii file CCF result tbl Fits files generic name e2ds A fits Fits files generic name e2ds B fits Fits files generic name s1d A fits Fits files generic name s1d B fits Fits files generic name ccf mask A fits Fits files generic name cc mask A tbl Quality control Warning if saturation level reached 3M6 MAN HAR 33110 0016 Issue 1 0 15 3 2 9 obj TWO Spectroscopy using Two fibers Inputs Raw fits frame obtained with the HARPS ech acq objAB template Description Retrieve from calibDB previous last full calibration sets Correction of the bad columns of the CCDs average of adjacent columns Correction of the BIAS as described previously Read the last localisation flat field wavelength solution and Thorium reference spectrum in the Calibration Data Base Horn optimum extraction of orders Flat field correction Save E2DS Thorium spectrum in FITS file with the suffix e2ds with all descriptors Compute the rebinned and merged spectrum SID and save it with the suffix 514 Compute the Barycentric Ea
18. fi ber mean rms N lines err rms L0 rms L1 rms L2 drift name of the night directory name of the corresponding raw frame fiber name A or B mean value of the final solution in mpixel rms on the final solution in mpixel number of lines used in the final solution internal error in the final solution in mpixel rms on Littrow at cut 1 in mpixel rms on Littrow at cut 42 in mpixel rms on Littrow at cut 43 in mpixel drift in m s compared to previous wavelength solution 3M6 MAN HAR 33110 0016 Issue 1 0 Rflux flux ration by comparison with the previous solution Ccosmic number of corrected cosmic IM ref wavelenth of reference line 1 ampll ref amplitude in e of the reference line 1 Il2ref wavelenth of reference line 2 ampl2ref amplitude in e of the reference line 2 error spe estimate of the velocity photon noise error of the spectrum 4 3 6 drift result tbl column description night name of the night directory e2ds file name name of the corresponding thorium e2ds spectrum reference name of the thorium e2ds spectrum used as reference exp time exposure time s VR drift Instrumental Drift m s To Add to the CCF result Nbcosmic Nb cosmic corrected Flu ratio Flux ratio between thorium spectrum and reference Nborders killed Nb order killed by the process 4 3 7 CCF_result tbl column description night name name of the night directory file name name of the corresponding thorium e2ds spectrum
19. ication the modules used by the Data Reduction programs and their field of 3M6 MAN HAR 33110 0016 Issue 1 0 module name description hadmrBIAS Bias Measurement and Correction hadmrCDB Calibration Database access functions hadmrDARK Dark Measurement and correction functions hadmrEXTOR _ Extraction of Orders hadmrFITS Manipulate FITS hadmrFLAT Flat field Measurement and correction functions hadmrLOCOR Localization of orders hadmrRV Calculation of velocity Earth drift stellar hadmrTHORCA Thorium Calibration hadgtVISU Graphical functions hadgtMATH Mathematical functions Table 2 3 List of the modules used by the Reduction programs Chapter 3 On line DRS Description 3 1 Overview The On line Data Reduction is automatically executed with the Trigger which can be started by typing the command trig csh online on the whadrs under user haprs 3 2 Recipes Recipes are made of specific functions available in the Modules specifically developed for the HARPS DRS see Table 2 3 or part of the distribution of python modules see in section 2 5 Dependencies between recipes and modules can be found in the DRS design document We present in this chapter a description of the reduction task carried out by each recipes 3 2 1 cal BIAS CCD BIAS Inputs Raw fits frame obtained with the HARPS ech bias template Description Read keywords related to the CCDs parameters readout mode readout noise gain Correction
20. if found greater calibDB is not updated 3 2 6 cal 12 I spectrum measurement Inputs Raw fits frame obtained with the HARPS ech cal tunAD2 template Description Retreive from calibDB previous last full calibration sets Correction of the bad columns of the CCDs average of adjacent columns Correction of the BIAS as described previously Read the last localisation flat field and wavelength solution in the Calibration Data Base Horn optimum extraction of orders Flat field correction Save E2DS Thorium spectrum in FITS file with the suffix e2ds with all descriptors Outputs Fits files generic name e2ds A fits Quality control Error if saturation level reached on I spectrum DRS stops 3 2 7 obj TH Accurate RV measurement Inputs Raw fits frame obtained with the HARPS ech acq thosimult template Description Retreive from calibDB previous last full calibration sets Correction of the bad columns of the CCDs average of adjacent columns Correction of the BIAS as described previously Read the last localisation flat field wavelength solution and Thorium reference spectrum in the Calibration Data Base Horn optimum extraction of orders Flat field correction Save E2DS Thorium spectrum in FITS file with the suffix e2ds with all descriptors Compute the rebinned and merged spectrum S1D and save it with the suffix 514 Compute the instrumental drift with the Thorium spectrum relative to the last Thori
21. ince their format is completely compatible with Midas or other tools 5 2 Recipe 5 2 1 off visu e2ds Display E2DS order off visu e2ds py night e2dsfits order number ps night Night directory 2002 02 11 e2dsfi ts E2DS fits file HARPS 2002 02 11T20 13 45 768 e2ds A fits order number Order number 0 71 default value 49 ps Poscript file output option 0 1 default value 0 5 2 2 off visu 51 Display SID spectrum off visu sld py night sldfits lambda start lambda end ps 29 30 3M6 MAN HAR 33110 0016 Issue 1 0 night Night directory 2002 02 11 s1dfi ts S1d fits file HARPS 2002 02 11T20 13 45 768 sld A fits lambda start First wavelentgh Angstrom default value 3780 lambda end Last wavelentgh Angstrom default value 6912 ps Poscript file output option 0 1 it default value 0 5 2 3 off visu ccf Display CCF off visu ccf py night ccffits ps night The night directory 2002 02 11 ccffi ts CCf fits file HARPS 2002 02 11T20 13 45 768 G2 A fits ps Poscript file output option 0 1 it default value 0 5 2 4 off visu SN Display S N per orders off visu SN py night e2dsfits ps night The night directory 2002 02 11 e2dsfi ts CCf fits file HARPS 2002 02 11T20 13 45 768 e2ds A fits ps Poscript file output option 0 1 it default value 0 5 2 5 off visu rvo Display RV per orders off visu rvo py night ccftbl ps night The nigh
22. ipulation string e Fortran program interface f2py Most of these modules are part of the python 2 1 1 distribution version DRS is currently running on this version Some specific algorithm of the DRS are written in Fortran in order to increase the DRS execution 3M6 MAN HAR 33110 0016 Issue 1 0 7 They are included in Python library through the Fortran program interface 2py 2 6 Architecture of the DRS the directories and files related to the Data Reduction Software of HARPS are stored on the directory home harmgr From this point config docs scripts fortran python python f2pymodule python Recipes python Modules INTROOT DRS Contains all the Instrument Configuration Data files used by the DRS Contains all useful documents notes and manuals related to the DRS Contains all the executable programs or their links Contains all the fortran sources name f and their associated python modules namemodule sl Contains the python executable python csh and two initialization file startup py and startup recipes py Contains all the modules based on fortran code and their test python scripts Contains all the python reduction programs Contains all the python modules used by the reduction programs 2 7 Architecture of the DRS Modules the functions used by the reduction programs are grouped in modules related to a specific appli cation Table 2 3 describes all appl
23. le La Silla Maintenance Software Observatoire de Gen ve Observing Software Quality Control Quantum Efficiency Root Mean Square Read Out Noise Radial Velocity Radial Velocity per order Extracted 1 Dimension Spectra Signal to Noise Ratio Software To Be Defined To Be Completed Very Large Telescope 3M6 MAN HAR 33110 0016 Issue 1 0 Chapter 2 DRS Hardware and Software Environment 2 4 Overview The DRS runs on line on a dedicated HP UNIX Workstation whadrs The DRS deals with all the aspects of the scientific reduction of the raw data as well as the processing of these reduced data to extract the radial velocities The DRS does not interfere with the operation of the instrument i e observations are independent from the Data Reduction activity The DFS configuration is illustrated on Fig 2 1 and the DRS architecture on Fig 2 2 The DRS is designed to run automatically no user interaction like a batch process controlled by the Trigger see 3 right after the end of each exposure or at the completion of a sequence of exposures It is also possible to use a DRS off line to display and analyze reduced data 2 2 Architecture of the data on WHADRS The raw frames are automatically stored on the directory data raw YYYY MM DD where YYYY MM DD is the night directory automatically created at noon these directories are auto matically created by the DFS system at noon The reduced frames are auto
24. length calibration of the orders The row numbering of the matrix corresponds to the inverse of the column of the raw frame in order to have wavelength increasing with pixels see on Fig 4 1 The FITS descriptor includes all descriptors of the raw frame 4 2 6 Extracted two dimensional spectra _e2ds_ The extracted two dimensional spectra E2DS is a 4096 x Morder real matrix written on disk in FITS format with the 24 suffix added to the generic name Each line contains the extracted flux of one spectral order in photo electrons unit The line numbering of the matrix corresponds to the inverse of the column numbering of the raw frame in order to have wavelength increasing with pixels on E2DS format The FITS descriptor includes all descriptors of the raw frame The following extra descriptor HIERARCH ESO DRS related to the localization flat field Barycentric Earth Radial Velocity Instrumental drift and wavelength calibration are included CAL LOC FILE Localization file used string CAL EXT OPT Option extraction integer CAL EXT SIG Size extraction zone float CAL EXT COSM threshold cosmic detection float CAL EXT SNi S_N order center i float CAL EXT NBCOSi NbCos detected order i integer CAL FLAT WIN half size blaze window integer CAL FLAT FILE Flat file used string 3M6 MAN HAR 33110 0016 Issue 1 0 21 CAL FLAT NBFILES Nb of Flat files used integer CAL FLAT RMSi FF RMS order i float CAL ADDED NBRFILES Nb of raw fi
25. les processed integer CAL ADDED FILES Files name of raw files used string BERV Barycentric Earth Radial Velocity float BJD Barycentric Julian Day float BERVMX Maximum BERV float CAL TH FILE Wavelength file used string DRIFT REF FILE Th Drift ref file used string DRIFT VR Th RV Drift m s float DRIFT NBCOS Th Drift Nbr cosmic detected integer DRIFT RFLUX Th Drift Flux ratio float DRIFT NBORDKILL Th Drift Nb orders killed integer DRIFT NOISE Th Drift photon noise m s float CAL TH ORDER NBR nbr of orders in total int CAL TH ORDER START numbering of the first blue order int CAL TH ORDER NBLUE nbr of blue orders int CAL TH ORDER NGAP nbr of orders in the gap int CAL TH ORDER NRED nbr of red orders int CAL TH GUESS ORDER nbr of the first guess order int CAL TH GUESS LINES file name for first guess lines string CAL TH LINES file name for tbl of cal lines string CAL TH DEG LL degre polyn fit 11 x order int CAL TH DEG X degre polyn fit x Il order int CAL TH COEFF LL coeff for 11 x order dbl precision CAL TH COEFF X coeff for x ll order dbl precision 22 3M6 MAN HAR 33110 0016 Issue 1 0 The wavelength calibration f x order is related to the coefficient with the following equation A i o d 1 z 4 1 Ma A x 0 1 whered 2 ESO DRS CAL TH DEG LL bf A ESO DRS CAL TH COEFF LL and the inter nal numbering of the order raw number in the e2ds frame
26. list contains all the DRS parameters that are checked by the Quality Control process This list is stored on the config directory 4 4 3 Intrument Configuration Data Pool All the fixed parameters needed by the DRS are in the file hadmrICDP py on the directory con fig In this file one finds the characteristics of the CCD mapping of the FITS descriptor to DRS 28 3M6 MAN HAR 33110 0016 Issue 1 0 variable and all the parameters of DRS algorithms optimized for HARPS 4 4 4 Intrument Performance Database DRS outcome helpful to track instrument performance are stored on the table files cal BIAS result tbl cal DARK result tbl cal loc one result tbl cal FF result tbl andcal TH result tbl generic name spot thAB tbl generic name th lines A tbl generic name th lines B tbl Chapter 5 Off line DRS Description 5 1 Overview The Data Reduction Off line corresponds to a set of tools offer to the user through a Graphical User Interface to display and analyze the reduced data provided by the On line DRS The outputs of the Off line DRS are generated in the local directory Unfortunately the GUI of the Off line DRS has not been tested during the third commissioning and will not be available before January 2004 However users can send manually the off line recipes like commands following by parameters as described in the next section Note that these tools are not essential to analyze reduced data s
27. matically stored in the directory data reduced YYYY MM DD The calibration frames are copied in the calibration Data Base directory data calibDB The log files of the DRS are stored in the directory data msg 2 3 Execution of the On line DRS On line DRS is executed by a set of system commands recipes send automaticaly by the Trigger These recipes need two parameters 4 3M6 MAN HAR 33110 0016 Issue 1 0 WHARPS O 1 month Backup raw frames du OBs WHADHS qum raw frames DVD x raw frames reduced data logs WHADRS EE Ce Data Arch Unit DRS reduced data logs a Figure 2 1 DFS configuration RAW FRAMES Unit Calibration DB Reduced Data So PERFORMANCE CONFIG Figure 2 2 DRS architecture The DRS is control by the Trigger Products of the DRS are stored in Reduced Data A calibration data base Calibration DB is dynamically maintained by the DRS Performances and config files are static databases read only by the DRS where all relevant parameters useful for the DRS are stored CONFIG is used to stored parameters of algorithms and PERFORMANCE to store QC parameters 3M6 MAN HAR 33110 0016 Issue 1 0 5 Exposures type Templates Reduction program HARPS ech Recipes Calibration CCD BIAS 1 1_BIAS CCD Dark 1 l DARK Geometry of orders l 1 1 loc ONE Fl
28. mplate for each fibers A and B Description Retrieve from calibDB previous last full calibration sets Read keywords related to the CCDs pa rameters readout mode readout noise gain Read keywords related to the exposure type in order to determine the illuminated fiber Correction of the bad columns of the CCDs average of adjacent columns Correction of the BIAS determined in the 4 overscan areas The bias is determined for each of the 4096 rows by average of the 50 columns This skeem allow to conserve and correct the possible structure of the bias when the CCDs are illuminated Resize of the raw frame and cut through all the spectral orders on the central row of the CCD Renormalization the central row in order to put all orders at the same level Find all orders in the normalized central row greater than 0 15 This first step allow to find the 72 orders of fiber A and the 71 orders of fiber B listed in Table 6 1 From these starting points order position are searched and located by 20 pixel steps At each point profile of each order is fitted by a 3M6 MAN HAR 33110 0016 Issue 1 0 11 gaussian in order to measure its center and fwhm On the whole frame centers and FHWM of each order are determined on 200 points A 4th degrees polynome is fitted for each order to constrain the center and to measure its FWHM The typical RMS of the fit is 25 mpixels for the centering 75 mpixels for the fwhm The FWHM ranges of orders from
29. ors of the raw frame In addition the order position are stored with the following HIERARCH ESO DRS fits descriptor CAL LOC NBO number of orders localized int CAL LOC DEG degree of the polynomial fit 1nt CAL LOC CTRi Coeffi for center order 1i NBO x DEG float CAL LOC FWHMi for fwhm order 1 NBO x DEG float 4 2 3 Flat field frames flat The Flat field frame is a 4096 x norder real matrix written on disk in FITS format with the flat suffix added to the generic name Each lines contains the normalized flat field spectrum of the orders The row numbering of the matrix corresponds to the inverse of the column of the raw frame in order to have wavelength increasing with pixels see on Fig 4 1 The FITS descriptor includes all descriptors 20 3M6 MAN HAR 33110 0016 Issue 1 0 of the raw frame 4 2 4 Blaze frames blaze The Blaze frame is a 4096 x norder real matrix written on disk in FITS format with the _blaze_ suffix added to the generic name Each lines contains the pseudo blaze reponse of the orders The row numbering of the matrix corresponds to the inverse of the column of the raw frame in order to have wavelength increasing with pixels see on Fig 4 1 The FITS descriptor includes all descriptors of the raw frame 4 2 5 Wavelength frames wave The wavelength frame is a 4096 x norder real matrix written on disk in FITS format with the _wave_ suffix added to the generic name Each lines contains the wave
30. programs associated to each template types are listed in the table 2 1 The on line trigger is executed on the WHADRS workstation under user harps with the command trig csh online 6 3M6 MAN HAR 33110 0016 Issue 1 0 Description Reduction program Visualization Display one order of the E2DS spectrum off visu e2ds Display a domain of SID spectrum off visu sid Display SNR per orders off visu SN Display the CCF and its parameters Off visu ccf Display the RV per orders off visu rvo Radial velocity re computation Compute the CCF off newccf Table 2 2 List of off line data reduction programs 2 4 Execution of the Off line DRS The Off line DRS is used to display and analyze reduced data Off line DRS is executed by a set of system commands recipes send manually through a dedicated GUI or directly from the prompter The reduction programs associated to reduced datas are listed in the table 2 2 2 5 Programming language The programming language is Python a powerful object oriented interpreter programming lan guage that is easy to extend freely distributed and available for most computer platforms see http www python org and http www vex net parnassus The following python modules are needed by the DRS e Mathematical and Numerical Numeric e Graphical and visualization Gnuplot e FITS format manipulation pcfitsio fitsio e User interface Tkinter e system and files sys time shutil os e string man
31. rth Radial Velocity Compute the cross correlation function with a template mask driven by the spectral type for both fibers and save the average CCF on the fits file generic name ccf mask A fits the RV for each orders in the table generic name cc mask A tb1 and the summary of results on the ta ble CCF result tbl Outputs Ascii file CCF_result tbl Fits files generic name _e2ds_A fits Fits files generic name _e2ds_B fits Fits files generic name _s1d_A fits Fits files generic name _s1d_B fits Fits files generic name _ccf_mask_A fits Fits files generic name _ccf_mask_A tbl Fits files generic name _ccf_mask_B fits Fits files generic name _ccf_mask_B tbl Quality control Warning if saturation level reached 16 3M6 MAN HAR 33110 0016 Issue 1 0 Chapter 4 DRS Data Product Description 4 1 Data naming rules The raw frames are stored on FITS format by the DFS with the ESO VLT standard naming rules HARPS YYYY MM DDTHH MM SS SSS fits with YYYY MM DD and HH MM SS SSS being respectively the date and time of the begining of observation Image products of the DRS are stored on FITS format with the same generic names plus a additional suffix describing its format see next section for details and the specific fiber name A or B For example HARPS YYYY MM DDTHH MM SS SSS_e2ds_A fits is an E2DS format image of the fiber A product by the DRS from the HARPS YYYY MM DDTHH MM SS
32. t directory 2002 02 11 ceftbl Table CCF file HARPS 2002 02 11T20 13 45 768 ccf G2 A tbl ps Poscript file output option 0 1 it default value 0 3M6 MAN HAR 33110 0016 Issue 1 0 31 5 2 6 off newccf Re process CCF off newccf py night e2dsfits maskfilename targetRV widthccf stepccf night The night directory 2002 02 11 e2ds E2DS fits file HARPS 2002 02 11T20 13 45 768 e2ds A tbl maskfi lename Template of correlation K0 mas default is G2 mas targetRV Target Radial Velocity km s defaut is 0 widthccf Windows of the CFF km s default is 20 km s stepccf Step of the CCF km s default is 1 km s The new CCF is saved in the file generic name newwccf mask A fits 32 3M6 MAN HAR 33110 0016 Issue 1 0 Chapter 6 Use of the Data Archiving Unit This appendix describes the use of the Data Archiving Unit DAU This unit allows the VA to write his her data raw and reduced to DVD In order to archive the data of one night the following has to be done 1 Launch the Data Archiving Unit on the wharch machine as harps user with the command dau csh do not send it in a background process 2 Indicate the night date in the Night field the only one which is white pressing Enter key validates the entered value The process scan the corresponding night directory in the whadrs workstation and compute the size in MB 3 Select the Backup buttons of the data files you want to archive and
33. um reference in the Calibration Data Base and save the result in the file drift result tbl Compute the Barycentric Earth Radial Velocity Compute the cross correlation function with a template mask driven by the spectral type and save the average CCF on the fits file generic name cc mask A fits the RV for each orders in the table generic name cc mask A tb1 and the summary of results on the table CCF_result tbl Outputs Asciifile drift result tbl 14 3M6 MAN HAR 33110 0016 Issue 1 0 Ascii file CCF_result tbl Fits files generic name _e2ds_A fits Fits files generic name _e2ds_B fits Fits files generic name _s1d_A fits Fits files generic name _s1d_B fits Fits files generic name _ccf_mask_A fits Fits files generic name _ccf_mask_A tbl Quality control Warning if saturation level reached 3 2 8 obj ONE Spectroscopy using One fiber Inputs Raw fits frame obtained with the HARPS_ech_acq_objA template Description Retrieve from calibDB previous last full calibration sets Correction of the bad columns of the CCDs average of adjacent columns Correction of the BIAS as described previously Read the last localisation flat field wavelength solution and Thorium reference spectrum in the Calibration Data Base Horn optimum extraction of orders Flat field correction Save E2DS Thorium spectrum in FITS file with the suffix e2ds with all descriptors Compute the rebinned and merg
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